  Planet multiplicities are useful in constraining the formation and evolution
of planetary systems but usually difficult to constrain observationally. Here,
we develop a general method that can properly take into account the survey
incompleteness and recover the intrinsic planet multiplicity distribution. We
then apply it to the radial velocity (RV) planet sample from the California
Legacy Survey (CLS). Within the $1\,$au ($10\,$au) region, we find $21 \pm 4\%$
($19.2 \pm 2.8\%$) of Sun-like stars host planets with masses above
$10\,M_\oplus$ ($0.3\,M_{\rm J}$), about 30\% (40\%) of which are multi-planet
systems; in terms of the RV semi-amplitude $K$, $33 \pm 7\%$ ($25 \pm 3\%$) of
Sun-like stars contain planets of $K>1\,$m/s ($3\,$m/s), and each system hosts
on average $1.8 \pm 0.4$ ($1.63 \pm 0.16$) planets. We note that the hot
Jupiter rate in the CLS Sun-like sample is higher than the consensus value of
$\sim$1\% by a factor of about three. We also confirm previous studies on the
correlation between inner ($<1\,$au) and outer ($>1\,$au) planets.
