We present BIMA and SCUBA observations of the young cluster associated with BD + 40 \arcdeg~ { } 4124 in the dense molecular gas tracer CS J = 2 \rightarrow 1 and the continuum dust continuum at \lambda = 3.1 mm and \lambda = 850 \mu m. The dense gas and dust in the system is aligned into a long ridge morphology extending \sim 0.4 pc with 16 gas clumps of estimated masses ranging from 0.14 - 1.8 M _ { \odot } .
A north-south variation in the CS center line velocity can be explained with a two cloud model .
We posit that the BD + 40 \arcdeg~ { } 4124 stellar cluster formed from a cloud-cloud collision .
The largest linewidths occur near V1318 Cyg-S , a massive star affecting its natal environment .
In contrast , the dense gas near the other , more evolved , massive stars displays no evidence for disruption ; the material must either be processed into the star , dissipate , or relax , fairly quickly .
The more evolved low-mass protostars are more likely to be found near the massive stars .
If the majority of low-mass stars are coeval , the seemingly evolved low-mass protostars are not older : the massive stars have eroded their structures .
Finally , at the highest resolution , the \lambda = 3.1 mm dust emission is resolved into a flattened structure 3100 by 1500 AU with an estimated mass of 3.4 M _ { \odot } .
The continuum and CS emission are offset by 1 \farcs 1 from the southern binary source .
A simple estimate of the extinction due to the continuum emission structure is A _ { V } \sim 700 mag .
From the offset and as the southern source is detected in the optical , the continuum emission is from a previously unknown very young , intermediate-mass , embedded stellar object .