  The role of turbulent fragmentation in regulating the efficiency of star
formation in interstellar clouds is examined from new wide field imaging of
12CO and 13CO J=1-0 emission from the Rosette and G216-2.5 molecular clouds.
The Rosette molecular cloud is a typical star forming giant molecular cloud and
G215-2.5 is a massive molecular cloud with no OB stars and very little low mass
star formation. The properties of the turbulent gas flow are derived from the
set of eigenvectors and eigenimages generated by Principal Component Analysis
of the spectroscopic data cubes. While the two clouds represent quite divergent
states of star formation activity, the velocity structure functions for both
clouds are similar. The sonic scale, lambda_S, defined as the spatial scale at
which turbulent velocity fluctuations are equivalent to the local sound speed,
and the turbulent Mach number evaluated at 1 pc, M_{1pc}, are derived for an
ensemble of clouds including the Rosette and, G216-2.5 regions that span a
large range in star formation activity. We find no evidence for the positive
correlations between these quantities and the star formation efficiency, that
are predicted by turbulent fragmentation models. A correlation does exist
between the star formation efficiency and the sonic scale for a subset of
clouds with L_{FIR}/M(H_2) > 1 that are generating young stellar clusters.
Turbulent fragmentation must play a limited and non-exclusive role in
determining the yield of stellar masses within interstellar clouds.
