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We use 25 simulated galaxies from the NIHAO project to define andcharacterize a variety of kinematic stellar structures: thin and thick discs,large scale single discs, classical and pseudo bulges, spheroids, inner discs,and stellar haloes. These structures have masses, spins, shapes and rotationalsupport in good agreement with theoretical expectations and observational data.Above a dark matter halo mass of $2.5\times10^{\rm~11}M_{\rm\odot}$, allgalaxies have a classical bulge and 70\% have a thin and thick disc. Thekinematic (thin) discs follow a power-law relation between angular momentum andstellar mass $J_{\rm *}=3.4M_{\rm *}^{\rm1.26\pm0.06}$, in very good agreementwith the prediction based on the empirical stellar-to-halo mass relation in thesame mass range, and show a strong correlation between maximum `observed'rotation velocity and dark matter halo circular velocity $v_{\rm c}=6.4v_{\rmmax}^{0.64\pm0.04}$. Tracing back in time these structures' progenitors, wefind all to lose a fraction $1-f_j$ of their maximum angular momentum. Thindiscs are significantly better at retaining their high-redshift spins($f_j\sim0.70$) than thick ones ($f_j\sim0.40$). Stellar haloes have theirprogenitor baryons assembled the latest ($z_{\rm~1/2}\sim1.1$) and over thelongest timescales ($\tau\sim6.2$~Gyr), and have the smallest fraction of starsborn in-situ ($f_{\rm in-situ}=0.35\pm0.14$). All other structures have$1.5\lesssim z_{\rm1/2}\lesssim3$, $\tau=4\pm2$~Gyr and $f_{\rmin-situ}\gtrsim0.9$.

NIHAO XVI: The properties and evolution of kinematically selected discs, bulges and stellar haloes