  We present new observations of the Mystic Mountains cloud complex in the
Carina Nebula using the ALMA Atacama Compact Array (ACA) to quantify the impact
of strong UV radiation on the structure and kinematics of the gas. Our Band~6
observations target CO, $^{13}$CO, and C$^{18}$O; we also detect DCN J=3-2 and
$^{13}$CS J=5-4. A dendrogram analysis reveals that the Mystic Mountains are a
coherent structure, with continuous emission over $-$10.5 km s$^{-1}$ $<$ v <
$-$2 km s$^{-1}$. We perform multiple analyses to isolate non-thermal motions
in the Mystic Mountains including computing the turbulent driving parameter,
$b$, which indicates whether compressive or solenoidal modes dominate. Each
analysis yields values similar to other pillars in Carina that have been
observed in a similar way but are subject to an order of magnitude less intense
ionizing radiation. We find no clear correlation between the velocity or
turbulent structure of the gas and the incident radiation, in contrast to other
studies targeting different regions of Carina. This may reflect differences in
the initial densities of regions that go on to collapse into pillars and those
that still look like clouds or walls in the present day. Pre-existing
over-densities that enable pillar formation may also explain why star formation
in the pillars appears more evolved (from the presence of jets) than in other
heavily-irradiated but non-pillar-like regions. High resolution observations of
regions subject to an array of incident radiation are required to test this
hypothesis.
