  We have conducted an interferometric line survey in the 0.8 mm band toward
the young high-mass protostar candidate NGC 2264 CMM3 with ALMA. CMM3 is
resolved into the two continuum peaks, CMM3A and CMM3B, at an angular
separation of 0.9". Thus, CMM3 is found to be a binary system candidate. We
have detected molecular outflows associated with CMM3A and CMM3B each,
indicating active star formation. In addition to the two peaks, six faint
continuum peaks are detected around CMM3A and CMM3B, most of which are thought
to be evolved low-mass protostars. CMM3A is found to be rich in molecular line
emission including complex organic molecules such as HCOOCH3 and CH3OCH3. The
emission of complex organic molecules is distributed within a compact region
around the continuum peak of CMM3A. Hence, CMM3A apparently harbors a hot core.
On the other hand, CMM3B is deficient in molecular line emission, although its
continuum flux is almost comparable to that of CMM3A. Possible origins of the
striking difference between CMM3A and CMM3B are discussed.
