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We present a detailed investigation of the Large Magellanic Cloud (LMC) diskusing classical Cepheids. Our analysis is based on optical (I,V; OGLE-IV),near-infrared (NIR: J,H,Ks) and mid-infrared (MIR: w1; WISE) mean magnitudes.By adopting new templates to estimate the NIR mean magnitudes from single-epochmeasurements, we build the currently most accurate, largest and homogeneousmulti-band dataset of LMC Cepheids. We determine Cepheid individual distancesusing optical and NIR Period-Wesenheit relations (PWRs), to measure thegeometry of the LMC disk and its viewing angles. Cepheid distances based onoptical PWRs are precise at 3%, but accurate to 7, while the ones based on NIRPWRs are more accurate (to 3%), but less precise (2%-15%), given the higherphotometric error on the observed magnitudes. We found an inclination i=25.05$\pm$ 0.02 (stat.) $\pm$ 0.55 (syst.) deg, and a position angle of the lines ofnodes P.A.=150.76 $\pm$ 0.02(stat.) $\pm$ 0.07(syst.) deg. These values agreewell with estimates based either on young (Red Supergiants) or onintermediate-age (Asymptotic Giant Branch, Red Clump) stellar tracers, but theysignificantly differ from evaluations based on old (RR Lyrae) stellar tracers.This indicates that young/intermediate and old stellar populations havedifferent spatial distributions. Finally, by using the reddening-law fittingapproach, we provide a reddening map of the LMC disk which is ten times moreaccurate and two times larger than similar maps in the literature. We alsofound an LMC true distance modulus of $\mu_{0,LMC}=18.48 \pm 0.10$ (stat. andsyst.) mag, in excellent agreement with the currently most accurate measurement(Pietrzynski et al. 2013).

The panchromatic view of the Magellanic Clouds from Classical Cepheids. I. Distance, Reddening and Geometry of the Large Magellanic Cloud disk