  Context. This is the third of a series of papers devoted to study in detail
and with high-angular resolution intermediate-mass molecular outflows and their
powering sources. Aims. The aim of this paper is to study the intermediate-mass
YSO IRAS 20050+2720 and its molecular outflow, and put the results of this and
the previous studied sources in the context of intermediate-mass star
formation. Methods. We carried out VLA observations of the 7 mm continuum
emission, and OVRO observations of the 2.7 mm continuum emission, CO(1-0),
C18O(1-0), and HC3N(12-11) to map the core towards IRAS 20050+2720. The
high-angular resolution of the observations allowed us to derive the properties
of the dust emission, the molecular outflow, and the dense protostellar
envelope. By adding this source to the sample of intermediate-mass protostars
with outflows, we compare their properties and evolution with those of lower
mass counterparts. Results. The 2.7mm continuum emission has been resolved into
three sources, labeled OVRO 1, OVRO 2, and OVRO 3. Two of them, OVRO 1 and OVRO
2, have also been detected at 7 mm. OVRO 3, which is located close to the C18O
emission peak, could be associated with IRAS 20050+2720. The mass of the
sources, estimated from the dust continuum emission, is 6.5 Msun for OVRO 1,
1.8 Msun for OVRO 2, and 1.3 Msun for OVRO 3. The CO(1-0) emission traces two
bipolar outflows within the OVRO field of view, a roughly east-west bipolar
outflow, labeled A, driven by the intermediate-mass source OVRO 1, and a
northeast-southwest bipolar outflow, labeled B, probably powered by a YSO
engulfed in the circumstellar envelope surrounding OVRO 1.
