  We have conducted a survey of young single and multiple systems in the
Taurus-Auriga star-forming region with the Atacama Large Millimeter Array
(ALMA), substantially improving both the spatial resolution and sensitivity
with which individual protoplanetary disks in these systems have been observed.
These ALMA observations can resolve binary separations as small as 25--30 AU
and have an average 3$\sigma$ detection level of 0.35 mJy, equivalent to a disk
mass of $4 \times 10^{-5}$ M$_{\odot}$ for an M3 star. Our sample was
constructed from stars that have an infrared excess and/or signs of accretion
and have been classified as Class II. For the binary and higher order multiple
systems observed, we detect $\lambda = 1.3$ mm continuum emission from one or
more stars in all of our target systems. Combined with previous surveys of
Taurus, our 21 new detections increase the fraction of millimeter-detected
disks to over 75% in all categories of stars (singles, primaries, and
companions) earlier than spectral type M6 in the Class II sample. Given the
wealth of other information available for these stars, this has allowed us to
study the impact of multiplicity with a much larger sample. While millimeter
flux and disk mass are related to stellar mass as seen in previous studies, we
find that both primary and secondary stars in binary systems with separations
of 30 to 4200 AU have lower values of millimeter flux as a function of stellar
mass than single stars. We also find that for these systems, the circumstellar
disk around the primary star does not dominate the total disk mass in the
system and contains on average 62% of the total mass.
