  Previous studies of planet occurrence rates largely relied on photometric
stellar characterizations. In this paper, we present planet occurrence rates
for mid-type M dwarfs using spectroscopy, parallaxes, and photometry to
determine stellar characteristics. Our spectroscopic observations have allowed
us to constrain spectral type, temperatures, and in some cases metallicities
for 337 out of 561 probable mid-type M dwarfs in the primary Kepler field. We
use a random forest classifier to assign a spectral type to the remaining 224
stars. Combining our data with Gaia parallaxes, we compute precise ($\sim$3%)
stellar radii and masses, which we use to update planet parameters and planet
occurrence rates for Kepler mid-type M dwarfs. Within the Kepler field, there
are seven M3 V to M5 V stars which host 13 confirmed planets between 0.5 and
2.5 Earth radii and at orbital periods between 0.5 and 10 days. For this
population, we compute a planet occurrence rate of $1.19^{+0.70}_{-0.49}$
planets per star. For M3 V, M4 V, and M5 V, we compute planet occurrence rates
of $0.86^{+1.32}_{-0.68}$, $1.36^{+2.30}_{-1.02}$, and $3.07^{+5.49}_{-2.49}$
planets per star, respectively.
