  Intermediate-mass (IM) protostars provide a bridge between the low- and
high-mass protostars. Despite their relevance, little is known about their
chemical diversity. We want to investigate the molecular richness towards the
envelope of IM protostars and to compare their properties with other sources.
We have selected the isolated IM Class 0 protostar CepE-mm to carry out an
unbiased molecular survey with the IRAM 30m telescope between 72 and 350 GHz
with an angular resolution lying in the range 7-34". These data were
complemented with NOEMA observations of the spectral bands 85.9 - 89.6 GHz and
216.8 - 220.4 GHz at an angular resolution of 2.3 and 1.4", respectively. 30m
spectra show bright emission of O- and N-bearing COMs. We identify three
components in the spectral signature: an extremely broad line component
associated with the outflowing gas, a narrow line component associated with the
cold envelope, and a broad line component tracing the hot corino. NOEMA
observations reveal CepE-mm as a binary protostellar system CepE-A and B,
separated by 1.7". CepE-A dominates the core continuum emission and powers the
high-velocity jet associated with HH377. Our interferometric maps show that
COMs arises from a region of 0.7" size around CepE-A. Rotational temperatures
were found to lie in the range 20-40 K with column densities ranging from a few
10^15 cm-2 for O-bearing species, down to a few 10^14 cm-2 for N-bearing
species. Molecular abundances are similar to those measured towards other low-
and intermediate-mass protostars. High-mass hot cores are significantly less
abundant in methanol and N-bearing species are more abundant by 3 orders of
magnitude.CepE-mm reveals itself as a binary protostellar system with a strong
chemical differentiation. The brightest component of the binary is associated
with a hot corino. Its properties are similar to those of low-mass hot corinos.
