Context : 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 ^ { \prime \prime } 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 Sérsic 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 \pm 0.10 , an effective radius of R _ { e } = ( 5.1 \pm 1.0 ) pc , and a Sérsic index of n = 2.2 \pm 0.7 .
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 \pm 0.06 _ { sys } \pm 0.01 _ { 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 .