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 Spitzer and 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 ( \textgreater 1.83 \times 10 ^ { 2 } \mathrm { M _ { \odot } } ) , high linewidths ( v \textgreater 1.18 \mathrm { km / s } ) , and high mass densities ( \textgreater 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 .