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The Perseus Arm is the closest Galactic spiral arm from the Sun, offering anexcellent opportunity to study in detail its stellar population. However, itsdistance has been controversial with discrepancies by a factor of two.Kinematic distances are in the range 3.9-4.2 kpc as compared to 1.9-2.3 kpcfrom spectrophotometric and trigonometric parallaxes, reinforcing previousclaims that this arm exhibits peculiar velocities. We used the astrometricinformation of a sample of 31 OB stars from the star-forming W3 Complex toidentify another 37 W3 members and to derive its distance from their Gaia-DR2parallaxes with improved accuracy. The Gaia-DR2 distance to the W3Complex,2.14$^{+0.08}_{-0.07}$ kpc, coincides with the previous stellardistances of $\sim$ 2 kpc. The Gaia-DR2 parallaxes tentatively showdifferential distances for different parts of the W3 Complex: W3 Main, locatedto the NE direction, is at 2.30$^{+0.19}_{-0.16}$ kpc, the W3 Cluster (IC1795), in the central region of the complex, is at 2.17$^{+0.12}_{-0.11}$ kpc,and W3(OH) is at 2.00$^{+0.29}_{-0.23}$ kpc to the SW direction. The W3 Clusteris the oldest region, indicating that it triggered the formation of the othertwo star-forming regions located at the edges of an expanding shell around thecluster.

Gaia-DR2 distance to the W3 Complex in the Perseus Arm