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abstract: 'Historically, multiple populations in Globular Clusters (GCs) have been mostly studied from ultraviolet and optical filters down to stars that are more massive than $\sim$0.6$\mathcal{M}_{\odot}$. Here we exploit deep near-infrared (NIR) photometry from the [*Hubble Space Telescope*]{} to investigate multiple populations among M-dwarfs in the GC NGC6752. We discovered that the three main populations (A, B and C), previously observed in the brightest part of the color-magnitude diagram, define three distinct sequences that run from the main-sequence (MS) knee towards the bottom of the MS ($\sim$0.15 ${\mathcal M}_{\odot}$). These results, together with similar findings on NGC2808, M4, and $\omega$Centauri, demonstrate that multiple sequences of M-dwarfs are common features of the color-magnitude diagrams of GCs. The three sequences of low-mass stars in NGC6752 are consistent with stellar populations with different oxygen abundances. The range of \[O/Fe\] needed to reproduce the NIR CMD of NGC6752 is similar to the oxygen spread inferred from high-resolution spectroscopy of red-giant branch (RGB) stars. The relative numbers of stars in the three populations of M-dwarfs are similar to those derived among RGB and MS stars more massive than $\sim$0.6$\mathcal{M}_{\odot}$. As a consequence, the evidence that the properties of multiple populations do not depend on 