  We present low resolution, visible light spectra of 41 star clusters in the
spiral galaxy M101, taken with the Gemini/GMOS instrument. We measure Lick
indices for each cluster and compare with BaSTI models to estimate their ages
and metallicities. We also measure the line-of-sight velocities. We find that
25 of the clusters are fairly young massive clusters (YMCs) with ages of
hundreds of Myr, and 16 appear to be older, globular clusters (GCs). There are
at least four GCs with best fit ages of approximately 1-3 Gyr and eight with
best fit ages of approximately 5-10 Gyr. The mean metallicity of the YMCs is
[Fe/H] of approximately -0.1 and for the GCs is [Fe/H] of approximately -0.9.
We find a near-continuous spread in both age and metallicity for our sample,
which may indicate that M101 had a more-or-less continuous history of cluster
and star formation. From the kinematics, we find that the YMCs rotate with the
HI gas fairly well, while the GCs do not. We cannot definitively say whether
the GCs sampled here lie in an inner halo, thick disk, or bulge/psuedobulge
component, although given the very small bulge in M101, the last seems
unlikely. The kinematics and ages of the YMCs suggest that M101 may have
undergone heating of its disk or possibly a continuous merger/accretion history
for the galaxy.
