  We have derived high-spatial-resolution metallicity maps covering
$\sim$105~deg$^2$ across the Large Magellanic Cloud (LMC) using near-infrared
passbands from the VISTA Survey of the Magellanic Clouds. We attempt to
understand the metallicity distribution and gradients of the LMC up to a radius
of $\sim$ 6~kpc. We identify red giant branch (RGB) stars in spatially distinct
$Y, (Y-K_{\rm s})$ colour-magnitude diagrams. In any of our selected
subregions, the RGB slope is used as an indicator of the average metallicity,
based on calibration to metallicity using spectroscopic data. The mean LMC
metallicity is [Fe/H] = $-$0.42~dex ($\sigma$[Fe/H] = 0.04~dex). We find the
bar to be mildly metal-rich compared with the outer disc, showing evidence of a
shallow gradient in metallicity ($-0.008 \pm 0.001$ dex kpc$^{-1}$) from the
galaxy's centre to a radius of 6~kpc. Our results suggest that the LMC's
stellar bar is chemically similar to the bars found in large spiral galaxies.
The LMC's radial metallicity gradient is asymmetric. It is metal-poor and
flatter towards the southwest, in the direction of the Bridge. This hints at
mixing and/or distortion of the spatial metallicity distribution, presumably
caused by tidal interactions between the Magellanic Clouds.
