  We present results of a wide-field (approximately 60 x 90 pc) ALMA mosaic of
CO(2-1) and $^{13}$CO(2-1) emission from the molecular cloud associated with
the 30 Doradus star-forming region. Three main emission complexes, including
two forming a bowtie-shaped structure extending northeast and southwest from
the central R136 cluster, are resolved into complex filamentary networks.
Consistent with previous studies, we find that the central region of the cloud
has higher line widths at fixed size relative to the rest of the molecular
cloud and to other LMC clouds, indicating an enhanced level of turbulent
motions. However, there is no clear trend in gravitational boundedness (as
measured by the virial parameter) with distance from R136. Structures observed
in $^{13}$CO are spatially coincident with filaments and are close to a state
of virial equilibrium. In contrast, CO structures vary greatly in
virialization, with low CO surface brightness structures outside of the main
filamentary network being predominantly unbound. The low surface brightness
structures constitute ~10% of the measured CO luminosity; they may be shredded
remnants of previously star-forming gas clumps, or alternatively the
CO-emitting parts of more massive, CO-dark structures.
