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We present robust planet occurrence rates for Kepler planet candidates aroundM stars for planet radii $R_p = 0.5-4~\textrm{R}_\oplus$ and orbital periods $P= 0.5-256$ days using the approximate Bayesian computation (ABC) technique.This work incorporates the final Kepler DR25 planet candidate catalog and dataproducts and augments them with updated stellar properties using Gaia DR2 and2MASS PSC. We apply a set of selection criteria to select a sample of 1,746Kepler M dwarf targets that host 89 associated planet candidates. These early Mdwarfs and late K dwarfs were selected from cross-referenced targets usingseveral photometric quality flags from Gaia DR2 and color-magnitude cuts using2MASS magnitudes. We estimate a habitable zone occurrence rate of$f_{\textrm{M,HZ}} = 0.33^{+0.10}_{-0.12}$ for planets with $0.75-1.5$R$_\oplus$ size. We caution that occurrence rate estimates for Kepler M starsare sensitive to the choice of prior due to the small sample of target starsand planet candidates. For example, we find an occurrence rate of$4.2^{+0.6}_{-0.6}$ or $8.4^{+1.2}_{-1.1}$ planets per M dwarf (integratingover $R_p = 0.5-4~\textrm{R}_\oplus$ and $P = 0.5-256$ days) for our twochoices of prior. These occurrence rates are greater than those for FGK dwarftarget when compared at the same range of orbital periods, but similar tooccurrence rates when computed as a function of equivalent stellar insolation.Combining our result with recent studies of exoplanet architectures indicatesthat most, and potentially all, early-M dwarfs harbor planetary systems.

Occurrence Rates of Planets Orbiting M Stars: Applying ABC to Kepler DR25, Gaia DR2, and 2MASS Data