  [Abridged] We imaged a 2' x 2' region of the Orion Nebula cluster in 1.3 mm
wavelength continuum emission with the recently commissioned Combined Array for
Research in Millimeter Astronomy (CARMA) and with the Submillimeter Array
(SMA). Our mosaics include >250 known near-IR cluster members, of which 36 are
so-called "proplyds" that have been imaged previously with the Hubble Space
Telescope. We detected 40 sources in 1 mm continuum emission, and several of
them are spatially resolved with our observations. Dust masses inferred for
detected sources range from 0.01 to 0.5 Msun, and the average disk mass for
undetected sources is estimated to be ~0.001 Msun, approximately an order of
magnitude smaller than the minimum mass solar nebula. Most stars in the ONC
thus do not appear to currently possess sufficient mass in small dust grains to
form Jupiter-mass (or larger) planets. Comparison with previous results for
younger and older regions indicates that massive disks evolve significantly on
~Myr timescales. We also show that the percentage of stars in Orion surrounded
by disks more massive than ~0.01 Msun is substantially lower than in Taurus,
indicating that environment has an impact on the disk mass distribution.
Finally, we explore potential correlations of disk mass with stellar mass and
location within the cluster.
