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We present a 1.3 mm continuum survey of the young (2-3 Myr) stellar clusterIC 348, which lies at a distance of 310 pc, and is dominated by low-mass stars(M$_{\star}$ $\sim$ 0.1-0.6 M$_{\odot}$). We observed 136 Class II sources(disks that are optically thick in the infrared) at 0.8$''$ (200 au) resolutionwith a 3$\sigma$ sensitivity of $\sim$ 0.45 mJy (M$_{\rm dust}$ $\sim$ 1.3M$_{\oplus}$). We detect 40 of the targets and construct a mm-continuumluminosity function. We compare the disk mass distribution in IC 348 to thoseof younger and older regions, taking into account the dependence on stellarmass. We find a clear evolution in disk masses from 1 to 5-10 Myr. The diskmasses in IC 348 are significantly lower than those in Taurus (1-3 Myr) andLupus (1-3 Myr), similar to those of Chamaleon~I, (2-3 Myr) and $\sigma$ Ori(3-5 Myr) and significantly higher than in Upper Scorpius (5$-$10 Myr). About20 disks in our sample ($\sim$5$\%$ of the cluster members) have estimatedmasses (dust $+$ gas) $>$1 M$_{\rm Jup}$ and hence might be the precursors ofgiant planets in the cluster. Some of the most massive disks include transitionobjects with inner opacity holes based on their infrared SEDs. From a stackinganalysis of the 96 non-detections, we find that these disks have a typical dustmass of just $\lesssim$ 0.4 M$_{\oplus}$, even though the vast majority oftheir infrared SEDs remain optically thick and show little signs of evolution.Such low-mass disks may be the precursors of the small rocky planets found by\emph{Kepler} around M-type stars.

Alma Survey Of Circumstellar Disks In The Young Stellar Cluster IC 348