To better understand the star formation process it is necessary to
 examine the effects of environment on star-forming molecular clouds.
 The Magellanic Clouds provide environments very different from the
 Milky Way.  By studying star formation in the LMC and SMC we will
 gain insight into how varying environments affect star formation.
 A useful measure of the star formation going on in an individual
 molecular cloud is the far infrared luminosity from warm (~40 K)
 dust associated with embedded stellar objects.  Observations of
 the FIR luminosity will usually contain a significant contribution
 from cool (15-25 K) dust heated by the general ISRF.  In order to
 accurately measure the star formation from a cloud it is necessary
 to remove this cool dust component.  The cool dust spectrum peaks
 between 100 and 200 microns, therefore FIR data is needed in this
 range to obtain an accurate measure of star formation in molecular
 clouds.
     One way to quantify star formation in a molecular cloud is the
 star formation activity (SFA).  SFA is the ratio of FIR luminosity
 of the embedded sources to cloud mass.  We have already determined
 virial masses for several molecular clouds in the LMC and SMC using
 CO (J=1->0) observations. In addition we have mapped the clouds at
 60 and 100 microns using IRAS data.  ISO data will be used to
 determine the total FIR luminosity for several clouds in varying
 environments in the LMC, and in the SMC.  The ISO data is crucial
 in that it provides the long wavelength information needed to
 accurately measure the total FIR luminosity, as well as the cool
 dust component of this emission.