  The accuracy in determining the spatial-kinematical parameters of open
clusters makes them ideal tracers of the Galactic structure. Young open
clusters (YOCs) are the main representative of the clustered star formation
mode, which identifies how most of the stars in the Galaxy form. We apply the
Kriging technique to a sample of Gaia YOCs within a 3.5 kpc radius around the
Sun and log(age) $\leq$ 7.5, age in years, to obtain the $Z(X,Y)$ and
$V_Z(X,Y)$ maps. The previous work by Alfaro et al. (1991) showed that Kriging
can provide reliable results even with small data samples ($N \sim 100$). We
approach the 3D spatial and vertical velocity field structure of the Galactic
disk defined by YOCs and analyze the hierarchy of the stellar cluster
formation, which shows a rich hierarchical structure, displaying complexes
embedded within each other. We discuss the fundamental characteristics of the
methodology used to perform the mapping and point out the main results obtained
in phenomenological terms. Both the 3D spatial distribution and the vertical
velocity field reveal a complex disk structure with a high degree of
substructures. Their analysis provides clues about the main physical mechanisms
that shape the phase space of the clustered star formation in this Galactic
area. Warp, corrugations, and high local deviations in $Z$ and $V_Z$, appear
intimately connected in a single but intricate scenario.

Astrophysics of Galaxies