  We present a catalogue of 99 candidate clusters and groups of galaxies in the
redshift range 0.1 < z_{phot} < 1.3 discovered in the Spitzer First Look Survey
(FLS). The clusters are selected by their R - 3.6um galaxy color-magnitude
relation using the cluster red sequence algorithm. Using this cluster sample we
compute the 3.6um, 4.5um, 5.8um, & 8.0um cluster luminosity functions (LFs).
Similar to previous studies, we find that for the bands that trace stellar mass
at these redshifts (3.6um, 4.5um) the evolution in M* is consistent with a
passively evolving population of galaxies with a high formation redshift (z_{f}
> 1.5). Using the 3.6um LF as a proxy for stellar luminosity we remove this
component from the MIR (5.8um & 8.0um) cluster LFs and measure the LF of dusty
star formation/AGN in clusters. We find that at z < 0.4 the bright end of the
cluster 8.0um LF is well-described by a composite population of quiescent
galaxies and regular star forming galaxies with a mix consistent with typical
cluster blue fractions; however, at z > 0.4, an additional population of dusty
starburst galaxies is required to properly model the 8.0um LFs. Comparison to
field studies at similar redshifts shows a strong differential evolution in the
field and cluster 8.0um LFs with redshift. At z ~ 0.65 8.0um-detected galaxies
are more abundant in clusters compared to the field, but thereafter the number
of 8.0um sources in clusters declines with decreasing redshift and by z ~ 0.15,
clusters are underdense relative to the field by a factor of ~5. The rapid
differential evolution between the cluster and field LFs is qualitatively
consistent with recent field galaxy studies that show the star formation rates
of galaxies in high density environments are larger than those in low density
environments at higher redshift.
