ABSTRACT We present the first SkyMapper stellar population analysis of the Large Magellanic Cloud (hereafter LMC), including the identification of 3578 candidate Carbon Stars through their extremely red g − r colours. Coupled with Gaia astrometry, we analyse the distribution and kinematics of this Carbon Star population, finding the LMC to be centred at (RA, Dec.) = (80.90° ± 0.29, −68.74° ± 0.12), with a bulk proper motion of $(μ _{α },μ _{δ }) = (1.878± 0.007,0.293± 0.018) \, \mathrm{mas \, yr^{-1}}$ and a disc inclination of i = 25.6° ± 1.1 at position angle θ = 135.6° ± 3.3°. We complement this study with the identification and analysis of additional stellar populations, finding that the dynamical centre for red giant branch stars is similar to that seen for the Carbon Stars, whereas for young stars the dynamical centre is significantly offset from the older populations. This potentially indicates that the young stars were formed as a consequence of a strong tidal interaction, probably with the Small Magellanic Cloud. In terms of internal dynamics, the tangential velocity profile increases linearly within $∼ \!3\ \, \mathrm{kpc}$, after which it maintains an approximately constant value of $V_{\mathrm{ rot}} = 83.6± 1.7 \, \mathrm{km \, s^{-1}}$ until $∼ \!7 \, \mathrm{kpc}$. With an asymmetric drift correction, we estimate the mass within $7\, \mathrm{kpc}$ to be $M_{\rm LMC}(\lt 7\, \mathrm{kpc}) = (2.5± 0.1)\times 10^{10}{\rm \, {\rm M}_{⊙ }}$ and within the tidal radius ($∼\! 30\ \, \mathrm{kpc}$) to be $M_{\rm LMC}(\lt 30\, \mathrm{kpc}) = (1.06 ± 0.32)\times 10^{11}\ {\rm \, {\rm M}_{⊙ }}$, consistent with other recent measurements.