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We present a three-dimensional analysis of a sample of 22 859 type $ab$ RRLyrae stars in the Magellanic System from the OGLE-IV Collection of RR Lyraestars. The distance to each object was calculated based on its photometricmetallicity and a theoretical relation between color, absolute magnitude andmetallicity.  The LMC RR Lyrae distribution is very regular and does not show anysubstructures. We demonstrate that the bar found in previous studies may be anoverdensity caused by blending and crowding effects. The halo is asymmetricalwith a higher stellar density in its north-eastern area, which is also locatedcloser to us. Triaxial ellipsoids were fitted to surfaces of a constant numberdensity. Ellipsoids farther from the LMC center are less elongated and slightlyrotated toward the SMC. The inclination and position angle change significantlywith the $a$ axis size. The median axis ratio is $1:1.23:1.45$.  The RR Lyrae distribution in the SMC has a very regular, ellipsoidal shapeand does not show any substructures or asymmetries. All triaxial ellipsoidsfitted to surfaces of a constant number density have virtually the same shape(axis ratio) and are elongated along the line of sight. The median axis ratiois $1:1.10:2.13$. The inclination angle is very small and thus the positionangle is not well defined.  We present the distribution of RR Lyrae stars in the Magellanic Bridge area,showing that the Magellanic Clouds' halos overlap.  A comparison of the distributions of RR Lyrae stars and Classical Cepheidsshows that the former are significantly more spread and distributed regularly,while the latter are very clumped and form several distinct substructures.

OGLE-ing the Magellanic System: Three-Dimensional Structure of the Clouds and the Bridge Using RR Lyrae Stars