  We constrain the intrinsic architecture of Kepler planetary systems by
modeling the observed multiplicities of the transiting planets (tranets) and
their transit timing variations (TTVs). We robustly determine that the fraction
of Sun-like stars with Kepler-like planets, $\eta_{\rm Kepler}$, is $30\pm3\%$.
Here Kepler-like planets are planets that have radii $R_{\rm p} \gtrsim
R_\oplus$ and orbital periods $P<400$~days. Our result thus significantly
revises previous claims that more than 50\% of Sun-like stars have such
planets. Combining with the average number of Kepler planets per star
($\sim0.9$), we obtain that on average each planetary system has $3.0\pm0.3$
planets within 400 days. We also find that the dispersion in orbital
inclinations of planets within a given planetary system, $\sigma_{i,k}$, is a
steep function of its number of planets, $k$. This can be parameterized as
$\sigma_{i,k}\propto k^\alpha$ and we find that $-4<\alpha<-2$ at 2-$\sigma$
level. Such a distribution well describes the observed multiplicities of both
tranets and TTVs with no excess of single tranets. Therefore we do not find
evidence supporting the so-called "Kepler dichotomy." Together with a previous
study on orbital eccentricities, we now have a consistent picture: the fewer
planets in a system, the hotter it is dynamically. We discuss briefly possible
scenarios that lead to such a trend. Despite our Solar system not belonging to
the Kepler club, it is interesting to notice that the Solar system also has
three planets within 400 days and that the inclination dispersion is similar to
Kepler systems of the same multiplicity.
