  We aim at characterizing a sample of 9 new hard X-ray selected Cataclysmic
Variable (CVs), to unambiguously identify them as magnetic systems of the
Intermediate Polar (IP) type. We performed timing and spectral analysis by
using X-ray, and simultaneous UV and optical data collected by XMM-Newton,
complemented with hard X-ray data provided by INTEGRAL and Swift. The pulse
arrival time were used to estimate the orbital periods. The X-ray spectra were
fitted using composite models consisting of different absorbing columns and
emission components. Strong X-ray pulses at the White Dwarf (WD) spin period
are detected and found to decrease with energy. Most sources are spin-dominated
systems in the X-rays, though four are beat dominated at optical wavelengths.
We estimated the orbital period in all system (except for IGR J16500-3307),
providing the first estimate for IGR J08390-4833, IGR J18308-1232, and IGR
J18173-2509. All X-ray spectra are multi-temperature. V2069 Cyg and RX
J0636+3535 posses a soft X-ray optically thick component at kT 80 eV. An
intense K_alpha Fe line at 6.4 keV is detected in all sources. An absorption
edge at 0.76 keV from OVII is detected in IGR J08390-4833. The WD masses and
lower limits to the accretion rates are estimated. We found all sources to be
IPs. IGR J08390-4833, V2069 Cyg, and IGR J16500-3307 are pure disc accretors,
while IGR J18308-1232, IGR J1509-6649, IGR J17195-4100, and RX J0636+3535
display a disc-overflow accretion mode. All sources show a temperature gradient
in the post-shock regions and a highly absorbed emission from material located
in the pre-shock flow which is also responsible for the X-ray pulsations.
Reflection at the WD surface is likely the origin of the fluorescent iron line.
There is an increasing evidence for the presence of a warm absorber in IPs. The
addition of 2 systems to the subgroup of soft X-ray IPs confirms a \sim 30%
incidence.
