  We have analyzed Chandra archival observations of the Antennae galaxies to
study the distribution and physical properties of its hot interstellar gas.
Eleven distinct diffuse X-ray emission regions are selected according to their
underlying interstellar structures and star formation activity. The X-ray
spectra of these regions are used to determine their thermal energy contents
and cooling timescales. Young star clusters in these regions are also
identified and their photometric measurements are compared to evolutionary
stellar population synthesis models to assess their masses and ages. The
cluster properties are then used to determine the stellar wind and supernova
energies injected into the ISM. Comparisons between the thermal energy in the
hot ISM and the expected stellar energy input show that young star clusters are
sufficient to power the X-ray-emitting gas in some, but not all, active star
formation regions. Super-star clusters, with masses >= 1x10^5 M_sol, heat the
ISM, but the yield of hot interstellar gas is not directly proportional to the
cluster mass. Finally, there exist diffuse X-ray emission regions which do not
show active star formation or massive young star clusters. These regions may be
powered by field stars or low-mass clusters formed within the last ~100 Myr.
