  We present deep CCD photometry of the very rich, intermediate aged (similar
to the Hyades) open star cluster NGC 2099 (M37). The V, B-V color-magnitude
diagram (CMD) for the cluster shows an extremely well populated and very
tightly constrained main-sequence extending over 12 magnitudes from the
turn-off. The CFH12K photometry for this cluster is faint enough (V ~ 24.5) to
detect the remnants of the most massive progenitor cluster stars under the Type
I SNe limit. Therefore, the CMD of the cluster also exhibits a well defined
white dwarf `clump' caused by the decreased rate of cooling of these stars as
they age, and a subsequent gap with very few objects. The termination point (Mv
= 11.95 +/- 0.30) of the white dwarf luminosity function gives a white dwarf
cooling age of 566 +/- 154/176 Myrs which is in excellent agreement with the
main-sequence turn-off isochrone age (520 Myrs). By carefully accounting for
errors, we show that the cooling age confirms that models including convective
core overshooting are preferred for young-intermediate aged clusters. We also
derive the reddening (E(B-V) = 0.21 +/- 0.03) and distance ((m-M)v = 11.55 +/-
0.13) to NGC 2099 by matching main-sequence features in the cluster to a new
fiducial main-sequence for the Hyades. As a continuing part of the goals of the
CFHT Open Star Cluster Survey to better understand dynamical processes of open
clusters, we also fit a King model to the cluster density distribution and
investigate the cluster main-sequence luminosity and mass functions in
increasing concentric annuli. We find some evidence for mass segregation within
the boundary of NGC 2099 as expected given the cluster's age relative to the
dynamical age. The present global mass function for the cluster is found to be
shallower than a Salpeter IMF.
