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We present $\mathrm{^{12}CO}$ and $\mathrm{^{13}CO}$ molecular gas dataobserved by ALMA, massive early stage young stellar objects identified byapplying color-magnitude cuts to \textit{Spitzer} and \textit{Herschel}photometry, and low-mass late stage young stellar objects identified viaH$\mathrm{\alpha}$ excess. Using dendrograms, we derive properties for themolecular cloud structures. This is the first time a dendrogram analysis hasbeen applied to extragalactic clouds. The majority of clumps have a virialparameter equal to unity or less. The size-linewidth relations of$\mathrm{^{12}CO}$ and $\mathrm{^{13}CO}$ show the clumps in this study have alarger linewidth for a given size (by factor of 3.8 and 2.5, respectively) incomparison to several, but not all, previous studies. The larger linewidths in30 Doradus compared to typical Milky Way quiescent clumps are probably due tothe highly energetic environmental conditions of 30 Doradus. The slope of thesize-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 consistentwithin 3$\mathrm{\sigma}$ of previous studies. Massive star formation occurs inclumps with high masses ($> 1.83 \times 10^{2}\;\mathrm{M_{\odot}}$), highlinewidths (v $> 1.18\;\mathrm{km/s}$), and high mass densities ($> 6.67 \times10^{2}\;\mathrm{M_{\odot}\;pc^{-2}}$). The majority of embedded, massive youngstellar objects are associated with a clump. However the majority of moreevolved, low-mass young stellar objects are not associated with a clump.

Studying Relation Between Star Formation and Molecular Clumps on Subparsec Scales in 30 Doradus