  Recent advances in our understanding of massive star formation have made
clear the important role of protostellar disks in mediating accretion. Here we
describe a simple, semi-analytic model for young, deeply embedded, massive
accretion disks. Our approach enables us to sample a wide parameter space of
stellar mass and environmental variables, providing a means to make predictions
for a variety of sources that next generation telescopes like ALMA and the EVLA
will observe. Moreover we include, at least approximately, multiple mechanisms
for angular momentum transport, a comprehensive model for disk heating and
cooling, and a realistic estimate for the angular momentum in the gas
reservoir. We make predictions for the typical sizes, masses, and temperatures
of the disks, and describe the role of gravitational instabilities in
determining the binarity fraction and upper mass cut-off.
