  We report on the results of a time-series photometric survey of NGC 2362,
carried out using the CTIO 4m Blanco telescope and Mosaic-II detector as part
of the Monitor project. Rotation periods were derived for 271 candidate cluster
members over the mass range 0.1 <~ M/Msol <~ 1.2. The rotation period
distributions show a clear mass-dependent morphology, qualitatively similar to
that in NGC 2264, as would be expected from the age of this cluster. Using
models of angular momentum evolution, we show that angular momentum losses over
the ~1-5 Myr age range appear to be needed in order to reproduce the evolution
of the slowest rotators in the sample from the ONC to NGC 2362, as found by
many previous studies. By incorporating Spitzer IRAC mid-IR measurements, we
found that 3-4 objects showing mid-IR excesses indicative of the presence of
circumstellar discs were all slow rotators, as would be expected in the disc
regulation paradigm for early pre-main sequence angular momentum evolution, but
this result is not statistically significant at present, given the extremely
limited sample size.
