  A large scale, high resolution map of CO(1-0) emission toward the OMC-2 and
OMC-3 star forming regions is presented. The map is a mosaic of 46 fields using
the Berkeley-Illinois-Maryland Array (BIMA) and covers $\sim 10'\times 15'$ at
$\sim 10" $ resolution. These data are combined with singledish FCRAO
observations and analyzed to identify and determine the properties of nine
protostellar outflows. The BIMA data alone almost completely resolve out the
cloud emission at central velocities and only recover 1/20 of the flux in the
high velocity gas showing that outflows are generally broadly dispersed over
$\sim 1'$ angular scales. All nine identified outflows emanate from known Class
0 or borderline Class 0/I sources, are associated with knots of shocked \h2\
emission, and have short dynamical times. It is suggested that only the
youngest, most spatially compact, and energetic outflows have been found and
that more distributed high velocity gas undetected by BIMA is due to older
outflows continuing through the Class I phase of protostellar evolution. The
mechanical energy injection rate into the cloud is estimated to be $\sim 1.5
L_\odot$ which is comparable to the turbulent energy dissipation rate.
Outf`lows appear capable, therefore, of sustaining cloud turbulence but a high
starformation rate is required implying a short cloud lifetime $\leq 5$ `Myr.
