  The ESO public survey VISTA Variables in the V\'ia L\'actea (VVV) has
contributed with deep multi-epoch photometry of the Galactic bulge and the
adjacent part of the disk over 526 square degrees. More than a hundred cluster
candidates have been reported thanks to this survey. We present the fifth
article in a series of papers focused on young and massive clusters discovered
in the VVV survey. In this paper, we present the physical characterization of
five clusters with a spectroscopically confirmed OB-type stellar population. To
characterize the clusters, we used near-infrared photometry ($J$, $H,$ and
$K_S$) from the VVV survey and near-infrared $K$-band spectroscopy from ISAAC
at VLT, following the methodology presented in the previous articles of the
series. All clusters in our sample are very young (ages between 1-20 Myr), and
their total mass are between $(1.07^{+0.40}_{-0.30})\cdot10^2$ $M_{\odot}$ and
$(4.17^{+4.15}_{-2.08})\cdot10^3$ $M_{\odot}$. We observed a relation between
the clusters total mass $M_{ecl}$ and the mass of their most massive stellar
member $m_{max}$, even for clusters with an age $<$ 10 Myr.
