  High-resolution ($<$0.1pc) ALMA observations of the 30Dor-10 molecular cloud
15pc north of R136 are presented. The $^{12}$CO 2-1 emission morphology
contains clumps near the locations of known mid-infrared massive protostars, as
well as a series of parsec-long filaments oriented almost directly towards
R136. There is elevated kinetic energy (linewidths at a given size scale) in
30Dor-10 compared to other LMC and Galactic star formation regions, consistent
with large scale energy injection to the region. Analysis of the cloud
substructures is performed by segmenting emission into disjoint approximately
round "cores" using clumpfind, by considering the hierarchical structures
defined by isointensity contours using dendrograms, and by segmenting into
disjoint long thin "filaments" using Filfinder. Identified filaments have
widths $\sim$0.1pc. The inferred balance between gravity and kinematic motions
depends on the segmentation method: Entire objects identified with clumpfind
are consistent with free-fall collapse or virial equilibrium with moderate
external pressure, whereas many dendrogram-identified parts of hierarchical
structures have higher mass surface densities $\Sigma_{LTE}$ than if
gravitational and kinetic energies were in balance. Filaments have line masses
that vary widely compared to the critical line mass calculated assuming thermal
and nonthermal support. Velocity gradients in the region do not show any strong
evidence for accretion of mass along filaments. The upper end of the "core"
mass distribution is consistent with a power-law with the same slope as the
stellar initial mass function.
