  The Milky Way nuclear star cluster (MWNSC) is a crucial laboratory for
studying the galactic nuclei of other galaxies, but its properties have not
been determined unambiguously until now. Aims. We aim to study the size and
spatial structure of the MWNSC. Methods. This study uses data and methods that
address potential shortcomings of previous studies on the topic. We use $0.2''$
angular resolution $K_{s}$ data to create a stellar density map in the central
$86.4$pc x $21$pc at the Galactic center. We include data from selected
adaptive-optics-assisted images obtained for the inner parsecs. In addition, we
use IRAC/Spitzer mid-infrared (MIR) images. We model the Galactic bulge and the
nuclear stellar disk in order to subtract them from the MWNSC. Finally, we fit
a S\'ersic model to the MWNSC and investigate its symmetry. Results. Our
results are consistent with previous work. The MWNSC is flattened with an axis
ratio of $q=0.71 \pm0.10$, an effective radius of $R_{e}=(5.1 \pm1.0)$ pc, and
a S\'ersic index of $n=2.2 \pm0.7$. Its major axis may be tilted out of the
Galactic plane by up to $-10$ degrees. The distribution of the giants brighter
than the Red Clump (RC) is found to be significantly flatter than the
distribution of the faint stars. We investigate the 3D structure of the central
stellar cusp using our results on the MWNSC structure on large scales to
constrain the deprojection of the measured stellar surface number density,
obtaining a value of the 3D inner power law of
$\gamma=1.38\pm0.06_{sys}\pm0.01_{stat}$. Conclusions. The MWNSC shares its
main properties with other extragalactic NSCs found in spiral galaxies. The
differences in the structure between bright giants and RC stars might be
related to the existence of not completely mixed populations of different ages.
This may hint at recent growth of the MWNSC through star formation or cluster
accretion.
