We present the first high-resolution sub-mm survey of both dust and gas for a large population of protoplanetary disks .
Characterizing fundamental properties of protoplanetary disks on a statistical level is critical to understanding how disks evolve into the diverse exoplanet population .
We use ALMA to survey 89 protoplanetary disks around stars with M _ { \ast } > 0.1 ~ { } M _ { \odot } in the young ( 1–3 Myr ) , nearby ( 150–200 pc ) Lupus complex .
Our observations cover the 890 \mu m continuum and the ^ { 13 } CO and C ^ { 18 } O 3–2 lines .
We use the sub-mm continuum to constrain M _ { dust } to a few Martian masses ( 0.2–0.4 M _ { \oplus } ) and the CO isotopologue lines to constrain M _ { gas } to roughly a Jupiter mass ( assuming ISM-like { [ CO ] / [ H _ { 2 } ] } abundance ) .
Of 89 sources , we detect 62 in continuum , 36 in ^ { 13 } CO , and 11 in C ^ { 18 } O at > 3 \sigma significance .
Stacking individually undetected sources limits their average dust mass to \lesssim 6 Lunar masses ( 0.03 M _ { \oplus } ) , indicating rapid evolution once disk clearing begins .
We find a positive correlation between M _ { dust } and M _ { \ast } , and present the first evidence for a positive correlation between M _ { gas } and M _ { \ast } , which may explain the dependence of giant planet frequency on host star mass .
The mean dust mass in Lupus is 3 \times higher than in Upper Sco , while the dust mass distributions in Lupus and Taurus are statistically indistinguishable .
Most detected disks have M _ { gas } \lesssim 1 ~ { } M _ { Jup } and gas-to-dust ratios < 100 , assuming ISM-like { [ CO ] / [ H _ { 2 } ] } abundance ; unless CO is very depleted , the inferred gas depletion indicates that planet formation is well underway by a few Myr and may explain the unexpected prevalence of super-Earths in the exoplanet population .