  We present $\mathrm{^{12}CO}$ and $\mathrm{^{13}CO}$ molecular gas data
observed by ALMA, massive early stage young stellar objects identified by
applying color-magnitude cuts to \textit{Spitzer} and \textit{Herschel}
photometry, and low-mass late stage young stellar objects identified via
H$\mathrm{\alpha}$ excess. Using dendrograms, we derive properties for the
molecular cloud structures. This is the first time a dendrogram analysis has
been applied to extragalactic clouds. The majority of clumps have a virial
parameter equal to unity or less. The size-linewidth relations of
$\mathrm{^{12}CO}$ and $\mathrm{^{13}CO}$ show the clumps in this study have a
larger linewidth for a given size (by factor of 3.8 and 2.5, respectively) in
comparison to several, but not all, previous studies. The larger linewidths in
30 Doradus compared to typical Milky Way quiescent clumps are probably due to
the highly energetic environmental conditions of 30 Doradus. The slope of the
size-linewidth relations of $\mathrm{^{12}CO}$, 0.65 $\pm$ 0.04, and
$\mathrm{^{13}CO}$, 0.97 $\pm$ 0.12, are on the higher end but consistent
within 3$\mathrm{\sigma}$ of previous studies. Massive star formation occurs in
clumps with high masses ($> 1.83 \times 10^{2}\;\mathrm{M_{\odot}}$), high
linewidths (v $> 1.18\;\mathrm{km/s}$), and high mass densities ($> 6.67 \times
10^{2}\;\mathrm{M_{\odot}\;pc^{-2}}$). The majority of embedded, massive young
stellar objects are associated with a clump. However the majority of more
evolved, low-mass young stellar objects are not associated with a clump.
