Star clusters in M33. II. Global properties

We discuss the global physical properties of stellar clusters in M33 and co mpare them with LMC cluster properties. In a companion paper (Paper I) we h ave compiled the first unbiased, representative sample of star clusters for this galaxy from Hubble Space Telescope WFPC2 multiband images of 20 field s in M33, sampling a variety of environments from outer regions to spiral a rms and central regions, as well as a range of Galactocentric distances. In this paper we fit single-mass King models to cluster surface brightness pr ofiles and iind that clusters at all ages have well-relaxed density profile s. Core radii are found to be smaller on average than those of Galactic glo bular clusters and LMC populous clusters at similar magnitudes; Measurement s of integrated photometric properties for 60 clusters are also found in Pa per I. By comparing the integrated photometric measurements with evolutiona ry models and theoretical M/L-V ratios, we find that clusters formed contin uously in M33 from similar to 4 X 10(6)-10(10) yr and have masses between s imilar to 4 x 10(2) and 3 x 10(5) M.. There is a correlation between the ag es and masses of our clusters, the oldest objects being the most massive. T he global properties of the M33 clusters are compared with cluster systems of other Local Group galaxies;By studying the photometric properties (magni tudes and colors) of M33 clusters and comparing them with those of LMC clus ters, a global picture of the star formation history in these two galaxies emerges.