  We study the structure of the inner Milky Way using the latest data release
of the Vista Variables in Via Lactea (VVV) survey. The VVV is a deep
near-infrared, multi-colour photometric survey with a coverage of 300 square
degrees towards the Bulge/Bar. We use Red Clump (RC) stars to produce a
high-resolution dust map of the VVV's field of view. From de-reddened
colour-magnitude diagrams we select Red Giant Branch stars to investigate their
3D density distribution within the central 4 kpc. We demonstrate that our
best-fit parametric model of the Bulge density provides a good description of
the VVV data, with a median percentage residual of 5$\%$ over the fitted
region. The strongest of the otherwise low-level residuals are overdensities
associated with a low-latitude structure as well as the so-called X-shape
previously identified using the split RC. These additional components
contribute only $\sim5\%$ and $\sim7\%$ respectively to the Bulge mass budget.
The best-fit Bulge is `boxy' with an axis ratio of [1:0.44:0.31] and is rotated
with respect to the Sun-Galactic Centre line by at least $20^{\circ}$. We
provide an estimate of the total, full sky, mass of the Bulge of
$M_\mathrm{Bulge}^{\mathrm{Chabrier}} = 2.36 \times 10^{10} M_{\odot}$ for a
Chabrier initial mass function. We show there exists a strong degeneracy
between the viewing angle and the dispersion of the Red Clump absolute
magnitude distribution. The value of the latter is strongly dependent on the
assumptions made about the intrinsic luminosity function of the Bulge.
