  We aim at studying the cluster environment surrounding the UCHII region in
IRAS 20293+3952, a region in the first stages of formation of a cluster around
a high-mass star. BIMA and VLA were used to observe the 3 mm continuum,
N2H+(1-0), NH3(1,1) and (2,2), and CH3OH(2-1) emission of the surroundings of
the UCHII region. We studied the kinematics of the region and computed the
rotational temperature and column density maps by fitting the hyperfine
structure of N2H+ and NH3. The dense gas traced by N2H+ and NH3 shows two
different clouds, a main cloud to the east of the UCHII region, of 0.5 pc and
250 Msun, and a western cloud, of 0.15 pc and 30 Msun. The dust emission
reveals two strong components in the northern side of the main cloud,
associated with Young Stellar Objects (YSOs) driving molecular outflows, and
two fainter components in the southern side, with no signs of star forming
activity. Regarding the CH3OH, we found strong emission in a fork-like
structure associated with outflow B, as well as emission associated with
outflow A. The rotational temperature is higher in the northern side of the
main cloud, around 22 K, where there are most of the YSOs, than in the southern
side, around 16 K. There is strong chemical differentiation in the region,
since we determined low values of the NH3/N2H+ ratio, around 50, associated
with YSOs in the north of the main cloud, and high values, up to 300,
associated with cores with no detected YSOs, in the south of the main cloud.
Such a chemical differentiation is likely due to abundance/depletion effects.
Finally, interaction between the different sources in the region is important,
mainly through their UV radiation and outflows (abridged).
