  We report on temporal and spectral analysis of the INTEGRAL fast transient
candidate IGR J16328-4726 observed with Beppo SAX in 1998 and more recently
with INTEGRAL. The MECS X-ray data show a frequent micro activity typical of
the intermediate state of Supergiant Fast X-ray Transients and a weak flare
with duration of ~4.6 ks. The X-ray emission in the 1.5-10 keV energy range is
well described through the different time intervals by an absorbed power law
model. Comparing spectra from the lower emission level up to the peak of the
flare, we note that while the power-law photon index was constant (~2), the
absorption column density varied by a factor of up to ~6-7, reaching the value
of ~2x10^{23}cm^{-2} at the peak of the flare. Analysis of the long-term
INTEGRAL/IBIS light curve confirms and refines the proposed ~10.07 day period,
and the derived ephemeris places the Beppo SAX observations away from
periastron. Using the near and the mid-IR available observations, we
constructed a spectral infrared distribution for the counterpart of IGR
J16328-4726, allowing us to identify its counterpart as a High Mass OB type
star, and to classify this source as a firm HMXB. Following the standard clumpy
wind theory, we estimated the mass and the radius of the clump responsible of
the flare. The obtained values of M~4x10^{22}g and R~4.4x10^6 km are in
agreement with expected values from theoretical predictions.
