  We have observed the $^{12}$CO J=2-1, J=3-2, and $^{13}$CO J=2-1 lines in a
sample of seven giant molecular clouds in the Local Group spiral galaxy M33.
The $^{12}$CO/$^{13}$CO J=2-1 line ratio is constant across the entire sample,
while the observed $^{12}$CO J=3-2/J=2-1 line ratio has a weak dependence on
the star formation environment of the cloud, with large changes in the line
ratio seen only for clouds in the immediate vicinity of an extremely luminous
HII region. A large velocity gradient analysis indicates that clouds without
HII regions have temperatures of 10-20 K, clouds with HII regions have
temperatures of 15-100 K, and the cloud in the giant HII region has a
temperature of at least 100 K. Interestingly, the giant HII region appears
capable of raising the kinetic temperature of the molecular gas only for clouds
that are quite nearby ($< 100$ pc). The continuous change of physical
conditions across the observed range of star formation environments suggests
that the unusual physical conditions in the cloud in the giant HII region are
due to post-star formation changes in the molecular gas, rather than intrinsic
properties of the gas related to the formation of the giant HII region.
