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We exploit the unprecedented depth of integral field data from the KMOSUltra-deep Rotational Velocity Survey (KURVS) to analyse the strong (H$\alpha$)and forbidden ([NII], [SII]) emission line ratios in 22 main-sequence galaxiesat $z\approx1.5$. Using the [NII]/H$\alpha$ emission-line ratio we confirm thepresence of the stellar mass $-$ gas-phase metallicity relation at this epoch,with galaxies exhibiting on average 0.13$\pm$0.04 dex lower gas-phasemetallicity (12+log(O/H)$_{\rm M13}$=8.40$\pm$0.03) for a given stellar mass($\log_{10}$($M_{\rm *}$[$M_{\odot}$]=10.1$\pm$0.1) than local main-sequencegalaxies. We determine the galaxy-integrated [SII] doublet ratio, with a medianvalue of [SII]$\lambda$6716/$\lambda$6731=1.26$\pm$0.14 equivalent to anelectron density of log$_{10}$($n_{\rm e}$[cm$^{-3}$])=1.95$\pm$0.12. UtilisingCANDELS $HST$ multi-band imaging we define the pixel surface-mass andstar-formation rate density in each galaxy and spatially resolve thefundamental metallicity relation at $z\approx1.5$, finding an evolution of0.05$\pm$0.01 dex compared to the local relation. We quantify the intrinsicgas-phase metallicity gradient within the galaxies using the [NII]/H$\alpha$calibration, finding a median annuli-based gradient of$\Delta$Z/$\Delta$R=$-$0.015$\pm$0.005 dex kpc$^{-1}$. Finally we examine theazimuthal variations in gas-phase metallicity, which show a negativecorrelation with the galaxy integrated star-formation rate surface density($r_{\rm s}$=$-$0.40, $p_{\rm s}$=0.07) but no connection to the galaxieskinematic or morphological properties nor radial variations in stellar masssurface density or star formation rate surface density. This suggests both theradial and azimuthal variations in interstellar medium properties are connectedto the galaxy integrated density of recent star formation.

The resolved chemical abundance properties within the interstellar medium of star-forming galaxies at $\mathbf{ \textit{z} \approx 1.5}$