  We present near and mid-infrared photometry obtained with the Spitzer Space
Telescope of 300 known members of the IC348 cluster. We merge this photometry
with existing ground-based optical and near-infrared photometry in order to
construct optical-infrared spectral energy distributions (SEDs) for all the
cluster members and present a complete atlas of these SEDs. We employ these
observations to both investigate the frequency and nature of the circumstellar
disk population in the cluster. The observations are sufficiently sensitive to
enable the first detailed measurement of the disk frequency for very low mass
stars at the peak of the stellar IMF. Using measurements of infrared excess
between 3.6 and 8 microns we find the total frequency of disk-bearing stars in
the cluster to be 50 +/- 6%. However, only 30 +/- 4% of the member stars are
surrounded by optically thick, primordial disks, while the remaining
disk-bearing stars are surrounded by what appear to be optically thin,anemic
disks. The disk fraction appears to be a function of spectral type and stellar
mass. The disk longevity and thus conditions for planet formation appear to be
most favorable for stars which are of comparable mass to the sun. The optically
thick disks around later type (> M4) stars appear to be less flared than the
disks around earlier type stars. This may indicate a greater degree of dust
settling and a more advanced evolutionary state for the late M disk population.
Finally we find that the presence of an optically thick dust disk is correlated
with gaseous accretion as measured by the strength of Halpha emission. These
results suggest that it is more likely for dust disks to persist in the absence
of active gaseous accretion than for active accretion to persist in the absence
of dusty disks.
