  We present Markov Chain Monte Carlo radiative transfer modeling of a joint
ALMA 345 GHz and spectral energy distribution dataset for a sample of 97
protostellar disks from the VLA and ALMA Nascent Disk and Multiplicity Survey
of Orion Protostars. From this modeling, we derive disk and envelope properties
for each protostar, allowing us to examine the bulk properties of a population
of young protostars. We find that disks are small, with a median dust radius of
$ 29.4^{+ 4.1}_{- 2.7}$ au and a median dust mass of $ 5.8^{+ 4.6}_{- 2.7}$
M$_{\oplus}$. We find no statistically significant difference between most
properties of Class 0, I, and Flat Spectrum sources with the exception of
envelope dust mass and inclination. The distinction between inclination is an
indication that the Class 0/I/Flat Spectrum system may be difficult to tie
uniquely to the evolutionary state of protostars. When comparing with Class II
disk dust masses in Taurus from similar radiative transfer modeling, we further
find that the trend of disk dust mass decreasing from Class 0 to Class II disks
is no longer present, though it remains unclear whether such a comparison is
fair due to differences in star forming region and modeling techniques.
Moreover, the disks we model are broadly gravitationally stable. Finally, we
compare disk masses and radii with simulations of disk formation and find that
magnetohydrodynamical effects may be important for reproducing the observed
properties of disks.
