  We analyzed the 2.6-mm CO and 21-cm HI lines toward the Magellanic
superbubble 30 Doradus C, in order to reveal the associated molecular and
atomic gas. We uncovered five molecular clouds in a velocity range from 251 to
276 km s$^{-1}$ toward the western shell. The non-thermal X-rays are clearly
enhanced around the molecular clouds on a pc scale, suggesting possible
evidence for magnetic field amplification via shock-cloud interaction. The
thermal X-rays are brighter in the eastern shell, where there are no dense
molecular or atomic clouds, opposite to the western shell. The TeV $\gamma$-ray
distribution may spatially match the total interstellar proton column density
as well as the non-thermal X-rays. If the hadronic $\gamma$-ray is dominant,
the total energy of the cosmic-ray protons is at least $\sim1.2 \times 10^{50}$
erg with the estimated mean interstellar proton density $\sim60$ cm$^{-3}$. In
addition the $\gamma$-ray flux associated with the molecular cloud (e.g., MC3)
could be detected and resolved by the Cherenkov Telescope Array (CTA). This
should permit CTA to probe the diffusion of cosmic-rays into the associated
dense ISM.
