I was watching a youtube from early in the Kepler mission (Jon Jenkins ; 
http://www.youtube.com/watch?v=UNGviQ0LPDQ
 if you wanna look at it), and it set out the "critical questions" the 
mission (now unfortunately over) was intended to answer. I will essay to
 say what they found out, based on listening to a number of NASA and 
other science website lectures on the subject. 
- 
- Are terrestrial planets common or rare? 
 
 - 
- What are their sizes and orbital distances? 
 
-  How often are they in the habitable zone?
 
First,
 it's worth pointing out what Kepler was for and what it did in the 
broadest terms. It's a space telescope, in solar orbit, that looked at 
only one small patch of sky in the Constellation Cygnus, along the disk 
of the Milky Way. It critically examined the "sunlike" stars in that 
field of view out to an effective distance of about 3000 light years. 
That's 150,000 stars, more or less similar to the Sun. The point was to 
try to detect planets, and create some meaningful statistics about what 
it found. 
Turns out what I'll call terrestroid (i.e., small, rocky) planets (e.g., Mercury, Venus, Earth, Mars) are very common.
 Kepler's methodology, which is detection of transiting planets 
(crossing the disk of their star as seen from Earth) involves a 
selection effect: only quite flat ecliptic-plane systems are detected, 
and only something like 2 or 3% at most of stars viewed in the Kepler 
field of view will be oriented correctly for detection. Single stars are
 also heavily favored, because binary star planetary disks, even though 
the stars (it turns out) may often have planets, are unlikely to be flat
 enough to have transiting planets. 
Still, it's thought that the systems Kepler has and will have 
detected (once all the data is processed), are relatively well 
representative of sunlike star systems in general. They found that small
 rocky planets are actually much more common than gas giants (in the 
Solar System we have four of each; a typical system might have four or 
five dense rocky worlds and only 1 or 2 gas planets, and there is not a
 preference for the rocky worlds to be close in, as formerly thought). 
So, from this point of view, very roughly earthlike worlds should be 
common. The question is implicit, what percentage of sunlike stars have 
planets at all? ... and the answer seems to be most of them, although 
the exact percentage is not really clear from Kepler data. 
Unfortunately, the one type of planet that would be most interesting, 
which is small planets, in the habitable zone of sunlike stars, and with
 an orbital period approximately similar to Earth's, is a type that the 
mission did not detect well, because it didn't have a long enough time 
to form a good baseline. Based on what was seen, there's good reason to 
believe that such planets (between let's say .9 and 1.5 Earth diameters,
 and in the zone where water can be liquid on the surface) are not 
particularly rare. A rough (but informed) guess would be maybe 2 to 5% 
of sunlike stars have such a planet. 
Of note, in the Solar System Earth is the largest of the terrestroid
 planets, but in most of these systems, rocky planets larger than Earth,
 up to 2½ Earth diameters (still small enough NOT to have retained their
 hydrogen envelopes, like Neptune or Uranus), are common. Such planets 
have been widely labeled "super-Earths" in the popular scientific 
literature. Various models have been proposed for what the implications 
of the greater mass and size of these planets would be, but there's a 
good deal of uncertainty still. 
- What is their dependence on stellar properties? 
 
This
 question is less clearly answered. Kepler did not look at stars dimmer 
than about K5, nor brighter than F0, so it is intrinsically limited to a
 category of stars that are actually quite a bit brighter than 
most stars,
 which are red dwarfs, on average. Turns out (from other detection 
methods) that red dwarfs almost always have planets, and the sunlike 
stars mostly do, too. The "habitable zones" of dimmer stars are very 
narrow, so it remains likely that sunlike stars are a good deal more 
likely to have liquid water surface rocky planets than are much dimmer 
stars. But since dimmer stars (not only the M dwarfs but the 
dimmer-range sunlike dwarfs, say from G5 to K5) are more common, it's a 
safe bet that the median, or typical, earthlike world with seas, clouds,
 mountains, plate tectonics, etc., (let's call them "First Order 
Earthlike;" the presence of life being another matter), will orbit a 
star dimmer than the Sun. Just exactly how those numbers will work out 
is still somewhat uncertain. 
Binary stars do, it seems, often have planets (most of this 
information comes from other planet detection regimes), so it would 
appear that at least some earthlike worlds could be "Tattooines" 
(planets orbiting two closely separated stars), or could orbit one of 
two or more very widely separated stars in a single system (e.g., Alpha 
Centauri, where planets have been detected). But these, it seems safe to
 say, will be the exceptions: habitable planets are more likely to be 
found orbiting single stars, probably by a significant margin.   
- Bottom line question: Are we alone? 
Unfortunately,
 unless there's a big surprise in the final reports, it doesn't appear 
that Kepler is going to answer this question. There are a number of 
suggested methods of teasing from the data information about whether 
life could exist on a planet that's been detected. The atmosphere of a 
planet transiting a star can affect the spectrum of the star, and from 
that comparison such things as the presence of ozone in the atmosphere 
could theoretically be inferred. A planet, for example, that had both 
methane and ozone detectable in its atmosphere would be so seriously in 
chemical disequilibrium that, albeit controversially, such a detection 
would be widely accepted as definitive proof of the existence of life 
there.* But it hasn't been demonstrated, so far. So while Kepler does not
 provide any reason to infer that life is not likely, or not present on 
one or more of the detected worlds, it doesn't confirm that, either. As 
for the detection of intelligent life; well, not. Again, nothing to rule
 it out, but nothing to confirm it either. 
♦♦
*The point is that if chemicals that will react with each other strongly 
both exist in the atmosphere of a planet, one or both of them must be 
continuously replenished, and in the case of oxygen (which yields ozone 
in the stratosphere), that can pretty much only be life, at least over 
time... if there were only one such detection, it could be explained 
away by transitory geological phenomena, but if the signature were 
detected in several different instances, the conclusion would be that it
 could pretty much 
only be a biosignature.