  The formation of galaxies can be understood in terms of the assembly patterns
of each type of galactic component. To perform this kind of analysis, is
necessary to define some criteria to separate those components. Decomposition
methods based on dynamical properties are more physically motivated than
photometry-based ones. We use the unsupervised Gaussian Mixture model of
\texttt{galactic structure finder} to extract the components of a sub-sample of
galaxies with Milky Way-like masses from the EAGLE simulations. A clustering in
the space of first and second order dynamical moments of all identified
substructures reveals five types of galaxy components: thin and thick disks,
stellar halos, bulges and spheroids. We analyse the dynamical, morphological
and stellar population properties of these five component types, exploring to
what extent these properties correlate with each other, and how much they
depend on the total galaxy stellar and dark matter halo masses. All galaxies
contain a bulge, a stellar halo and a disk. 60% of objects host two disks (thin
and thick), and 68% host also a spheroid. The dynamical disk-to-total ratio
does not depend on stellar mass, but the median rotational velocities of the
two disks do. Thin disks are well separated in stellar ages, [Fe/H] and
$\alpha$-enhancement from the three dispersion-dominated components, while
thick disks are in between. Except for thin disks, all components show
correlations among their stellar population properties: older ages mean lower
metallicities and larger $\alpha$-enhancement. Finally, we quantify the weak
dependence of stellar population properties on each component's dynamics.
