  We present ALMA observations of 101 protoplanetary disks within the
star-forming region Lynds 1641 in the Orion Molecular Cloud A. Our observations
include 1.33 mm continuum emission and spectral windows covering the J=2-1
transition of $^{12}$CO, $^{13}$CO, and C$^{18}$O. We detect 89 protoplanetary
disks in the dust continuum at the 4$\sigma$ level ($\sim$88% detection rate)
and 31 in $^{12}$CO, 13 in $^{13}$CO, and 4 in C$^{18}$O. Our sample contains
23 transitional disks, 20 of which are detected in the continuum. We target
infrared-bright Class II objects, which biases our sample towards massive
disks. We determine dust masses or upper limits for all sources in our sample
and compare our sample to protostars in this region. We find a decrease in dust
mass with evolutionary state. We also compare this sample to other regions
surveyed in the (sub-)millimeter and find that Lynds 1641 has a relatively
massive dust disk population compared to regions of similar and older ages,
with a median dust mass of 11.1$^{+32.9}_{-4.6}$ $M_\oplus$ and 27% with dust
masses equal to or greater than the minimum solar nebula dust mass value of
$\sim$30 $M_\oplus$. We analyze the disk mass-accretion rate relationship in
this sample and find that the viscous disk lifetimes are similar to the age of
the region, however with a large spread. One object, [MGM2012] 512, shows
large-scale ($>$5000 AU) structure in both the dust continuum and the three gas
lines. We discuss potential origins for this emission, including an accretion
streamer with large dust grains.
