  Theories of planet formation give contradicting results of how frequent
close-in giant planets of intermediate mass stars (IMSs; $\rm 1.3\leq
M_{\star}\leq 3.2\,M_{\rm \odot}$) are. Some theories predict a high rate of
IMSs with close-in gas giants, while others predict a very low rate. Thus,
determining the frequency of close-in giant planets of IMSs is an important
test for theories of planet formation. We use the CoRoT survey to determine the
absolute frequency of IMSs that harbour at least one close-in giant planet and
compare it to that of solar-like stars. The CoRoT transit survey is ideal for
this purpose, because of its completeness for gas-giant planets with orbital
periods of less than 10 days and its large sample of main-sequence IMSs. We
present a high precision radial velocity follow-up programme and conclude on 17
promising transit candidates of IMSs, observed with CoRoT. We report the
detection of CoRoT-34b, a brown dwarf close to the hydrogen burning limit,
orbiting a 1.1 Gyr A-type main-sequence star. We also confirm two inflated
giant planets, CoRoT-35b, part of a possible planetary system around a
metal-poor star, and CoRoT-36b on a misaligned orbit. We find that $0.12 \pm
0.10\,\%$ of IMSs between $1.3\leq M_{\star}\leq 1.6 M_{\rm \odot}$ observed by
CoRoT do harbour at least one close-in giant planet. This is significantly
lower than the frequency ($0.70 \pm 0.16\,\%$) for solar-mass stars, as well as
the frequency of IMSs harbouring long-period planets ($\rm \sim 8\,\%$).
